Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/8089
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dc.contributor.authorRao, Khushboo K-
dc.contributor.authorVaidya, Kaushar-
dc.contributor.authorAgarwal, Manan-
dc.contributor.authorPanthi, Anju-
dc.contributor.authorJadhav, Vikrant V-
dc.date.accessioned2022-11-23T05:33:47Z-
dc.date.available2022-11-23T05:33:47Z-
dc.date.issued2022-10-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, Vol. 516, No. 2, pp. 2444–2454en_US
dc.identifier.issn1365-2966-
dc.identifier.urihttp://hdl.handle.net/2248/8089-
dc.descriptionRestricted Accessen_US
dc.description.abstractUltraviolet (UV) wavelength observations have made a significant contribution to our understanding of hot stellar populations of star clusters. Multiwavelength spectral energy distributions (SEDs) of stars, including ultraviolet observations, have proven to be an excellent tool for discovering unresolved hot companions in exotic stars such as blue straggler stars (BSS), thereby providing helpful clues to constrain their formation mechanisms. Melotte 66 is a 3.4 Gyr old open cluster located at a distance of 4810 pc. We identify the cluster members by applying the ML-MOC algorithm on Gaia EDR3 data. Based on our membership identification, we find 1162 members, including 14 BSS candidates, 2 yellow straggler candidates (YSS), and one subdwarf B candidate (sdB). We generated SEDs for 11 BSS candidates and the sdB candidate using Swift/UVOT data combined with other archival data in the optical and IR wavelengths. We discover a hot companion of one BSS candidate, BSS3, with temperature of 38 000+7000−6000−6000+7000 K, luminosity of 2.99+5.47−1.86−1.86+5.47 L⊙, and radius of 0.04+0.008−0.005−0.005+0.008 R⊙. This hot companion is a likely low-mass WD with an estimated mass of 0.24–0.44 M⊙. We report one BSS candidate, BSS6, as an Algol-type eclipsing binary with a period of 0.8006 d, based on the Gaia DR3 variability classification. We suggest that BSS3 is formed via either the Case A or Case B mass-transfer channel, whereas BSS6 is formed via the Case A mass transfer.en_US
dc.language.isoenen_US
dc.publisherOxford University Press on behalf of Royal Astronomical Societyen_US
dc.relation.urihttps://doi.org/10.1093/mnras/stac2241-
dc.rights© Royal Astronomical Society-
dc.subjectBinaries: eclipsingen_US
dc.subjectBlue stragglersen_US
dc.subjectStars: formationen_US
dc.subjectOpen clusters and associations: individual: Melotte 66en_US
dc.titleCharacterization of hot populations of Melotte 66 open cluster using Swift/UVOTen_US
dc.typeArticleen_US
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